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Simultaneous, Multi-Wavelength Variability Characterization of the Free-Floating Planetary Mass Object PSO J318.5-22

Research output: Contribution to journalArticle

  • Beth Biller
  • Johanna Vos
  • Esther Buenzli
  • Katelyn Allers
  • Mickaël Bonnefoy
  • Benjamin Charnay
  • Bruno Bézard
  • France Allard
  • Derek Homeier
  • Mariangela Bonavita
  • Wolfgang Brandner
  • Ian Crossfield
  • Trent Dupuy
  • Thomas Henning
  • Taisiya Kopytova
  • Michael C. Liu
  • Elena Manjavacas
  • Joshua Schlieder

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https://arxiv.org/abs/1712.03746
Original languageEnglish
Article number95
JournalAstronomical Journal
Volume155
Issue number2
DOIs
Publication statusPublished - 31 Jan 2018

Abstract

We present simultaneous Hubble Space Telescope (HST) WFC3+Spitzer IRAC variability monitoring for the highly variable young (~20 Myr) planetary-mass object PSO J318.5−22. Our simultaneous HST + Spitzer observations covered approximately two rotation periods with Spitzer and most of a rotation period with the HST. We derive a period of 8.6 ± 0.1 hr from the Spitzer light curve. Combining this period with the measured $v\sin i$ for this object, we find an inclination of 56fdg2 ± 8fdg1. We measure peak-to-trough variability amplitudes of 3.4% ± 0.1% for Spitzer Channel 2 and 4.4%–5.8% (typical 68% confidence errors of ~0.3%) in the near-IR bands (1.07–1.67 μm) covered by the WFC3 G141 prism—the mid-IR variability amplitude for PSO J318.5−22 is one of the highest variability amplitudes measured in the mid-IR for any brown dwarf or planetary-mass object. Additionally, we detect phase offsets ranging from 200° to 210° (typical error of ~4°) between synthesized near-IR light curves and the Spitzer mid-IR light curve, likely indicating depth-dependent longitudinal atmospheric structure in this atmosphere. The detection of similar variability amplitudes in wide spectral bands relative to absorption features suggests that the driver of the variability may be inhomogeneous clouds (perhaps a patchy haze layer over thick clouds), as opposed to hot spots or compositional inhomogeneities at the top-of-atmosphere level.

    Research areas

  • astro-ph.EP

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